The Lupus clouds - European Southern Observatory
... La Silla. The field measures 112′ × 126′ and is centered at α(2000) = 16 : 09 : 20, δ(2000) = −38 : 33. North is at the top and East to the left. The bottom part of the field covers the thick clouds containing HR 5999 and HR 6000 (the bright stars near the center of the bottom half of the field), cl ...
... La Silla. The field measures 112′ × 126′ and is centered at α(2000) = 16 : 09 : 20, δ(2000) = −38 : 33. North is at the top and East to the left. The bottom part of the field covers the thick clouds containing HR 5999 and HR 6000 (the bright stars near the center of the bottom half of the field), cl ...
Galaxies - hwchemistry
... of galaxies, however, they find that the measured masses are much larger than expected from the luminosities of the galaxies. • This seems to be true of most galaxies. – Measured masses of galaxies amount to 10 to 100 times more mass than you would expect from the appearance of galaxies. ...
... of galaxies, however, they find that the measured masses are much larger than expected from the luminosities of the galaxies. • This seems to be true of most galaxies. – Measured masses of galaxies amount to 10 to 100 times more mass than you would expect from the appearance of galaxies. ...
Unfolding the Milky Way bulge - International Max Planck Research
... the red dashed line shows the synthetic spectrum using the best fitting abundance as obtained from our procedure. . . . . . . . . . . . . . . . . . . . . . . . . . Abundance errors associated with the uncertainties in effective temperature (upper left), surface gravity (upper right), metallicity (lo ...
... the red dashed line shows the synthetic spectrum using the best fitting abundance as obtained from our procedure. . . . . . . . . . . . . . . . . . . . . . . . . . Abundance errors associated with the uncertainties in effective temperature (upper left), surface gravity (upper right), metallicity (lo ...
STARLAB
... Charioteer, Lepus the Hare, Draco, and the Pleiades. Look at these constellations using the Constellation Cylinder. Hand out arrow pointers and show their locations. Look at the Starfield Cylinder and try to locate the same constellations. After leaving STARLAB, hand out star maps, and show the prop ...
... Charioteer, Lepus the Hare, Draco, and the Pleiades. Look at these constellations using the Constellation Cylinder. Hand out arrow pointers and show their locations. Look at the Starfield Cylinder and try to locate the same constellations. After leaving STARLAB, hand out star maps, and show the prop ...
... Theory and observations point to a variety of processes that redistribute energy in disks. In Section 2, we review evidence that bars and ovals rearrange disk gas into outer rings, inner rings, and central mass concentrations. The resulting star formation produces a central stellar subsystem that ha ...
The most metal-poor galaxies
... solar neighbourhood and the halo differ in metallicity. The most metal-poor halo stars have heavy element abundances 10−4 times that of the Sun (Cayrel 1996) while stars in the Galactic centre may be three times more metal rich than the Sun. On the other hand, the large ionised complexes in the ISM ...
... solar neighbourhood and the halo differ in metallicity. The most metal-poor halo stars have heavy element abundances 10−4 times that of the Sun (Cayrel 1996) while stars in the Galactic centre may be three times more metal rich than the Sun. On the other hand, the large ionised complexes in the ISM ...
Communications in Asteroseismology
... Who is Michel Breger? You can find him on the Austrian Academy of Science’s website as: Mag. rer. soc. nat., Dr. phil., B. Sc., M.A., o. Prof. Michel Breger and that is impressive! (Although few of us have much idea what it all means.) He was born Michel (as pronounced in German with a guttural “ch”) ...
... Who is Michel Breger? You can find him on the Austrian Academy of Science’s website as: Mag. rer. soc. nat., Dr. phil., B. Sc., M.A., o. Prof. Michel Breger and that is impressive! (Although few of us have much idea what it all means.) He was born Michel (as pronounced in German with a guttural “ch”) ...
Differential rotation in Sun-like stars from surface variability and
... Stellar winds: Stars like the Sun exhibit a stellar wind which consists of charged particles that are thermally and centrifugally liberated from their coronae (Parker 1958). These particles are initially locked to the magnetic field lines out to a radius where the field strength becomes less than th ...
... Stellar winds: Stars like the Sun exhibit a stellar wind which consists of charged particles that are thermally and centrifugally liberated from their coronae (Parker 1958). These particles are initially locked to the magnetic field lines out to a radius where the field strength becomes less than th ...
A spectroscopic study of detached binary systems using precise radial velocities
... The orbital periods of these systems range from about 10 days to 26 years, with a median of about 6 years. Orbital solutions were determined for the seven systems with shorter periods. The measurement of the mass ratio of the longest-period system, HD 217166, demonstrates that this important astroph ...
... The orbital periods of these systems range from about 10 days to 26 years, with a median of about 6 years. Orbital solutions were determined for the seven systems with shorter periods. The measurement of the mass ratio of the longest-period system, HD 217166, demonstrates that this important astroph ...
Structure in the first quadrant of the Galaxy: an analysis of TMGS star
... which are available as Supplementary Material in the electronic version of MNRAS), we present TMGS counts along nine strips in the first quadrant. These illustrate our interpretations of the counts by direct comparisons with the predictions of SKY. Differential counts were scaled per square degree p ...
... which are available as Supplementary Material in the electronic version of MNRAS), we present TMGS counts along nine strips in the first quadrant. These illustrate our interpretations of the counts by direct comparisons with the predictions of SKY. Differential counts were scaled per square degree p ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... UBVRI images of 16 dwarf elliptical galaxies in the Virgo Cluster were obtained with the VATT 1.8m on 2003 March 29-31. The telescope was equipped with CCD26, a thinned Loral 3 2048 × 2048 CCD with 15µm pixels. CCD26 has a read noise of 5.7 e− and a gain of 1.9 e− per ADU was used. On-chip binning o ...
... UBVRI images of 16 dwarf elliptical galaxies in the Virgo Cluster were obtained with the VATT 1.8m on 2003 March 29-31. The telescope was equipped with CCD26, a thinned Loral 3 2048 × 2048 CCD with 15µm pixels. CCD26 has a read noise of 5.7 e− and a gain of 1.9 e− per ADU was used. On-chip binning o ...
- Isaac Newton Group of Telescopes
... of their evolution. More massive brown dwarfs in the Pleiades should be detectable in sufficiently deep surveys. After only 0.3% of the clusters area had been explored using IAC80 telescope at Teide Observatory, a faint object was detected, whose extremely red colour possibly indicated a very low s ...
... of their evolution. More massive brown dwarfs in the Pleiades should be detectable in sufficiently deep surveys. After only 0.3% of the clusters area had been explored using IAC80 telescope at Teide Observatory, a faint object was detected, whose extremely red colour possibly indicated a very low s ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.